منابع مشابه
The Energy Spectrum of Primary Cosmic Ray Electrons in Clusters of Galaxies and Inverse Compton Emission
Models for the evolution of the integrated energy spectrum of primary cosmic ray electrons in clusters of galaxies have been calculated, including the effects of losses due to inverse Compton (IC), synchrotron, and bremsstrahlung emission, and Coulomb losses to the intracluster medium (ICM). The combined time scale for these losses reaches a maximum of ∼3×109 yr for electrons with a Lorentz fac...
متن کاملCosmic - Ray Electrons and the Diffuse Gamma - Ray Spectrum
Short Title: Cosmic-ray electrons and diffuse gamma-ray spectrum 1 Abstract The bulk of the diffuse galactic gamma-ray emission above a few tens of GeV has been conventionally ascribed to the decay of neutral pions produced in cosmic-ray interactions with interstellar matter. Cosmic-ray electrons may, however, make a significant contribution to the gamma-ray spectrum at high energies, and even ...
متن کاملThe Local Interstellar Spectrum of Cosmic Ray Electrons
The direct measurements of electrons and positrons over the last 30 years, corrected for the solar effect in the force-field approximation, are considered. The resulting overall electron spectrum may be fitted with a single power law above few GeV with spectral index (γ− = 3.41 ± 0.02), consistent with the spectral index of the positron spectrum (γ+ = 3.40 ± 0.06), therefore suggesting a common...
متن کاملThe Local Interstellar Spectrum of Cosmic Ray Electrons . Direct measurements
The local interstellar spectrum of cosmic ray electrons is derived by correcting the data from balloon and space measurements for the solar modulation effect. The resulting spectrum, after the renormalization of some experimental data set, can be fitted with a single power law from about 3 GeV to 2 TeV with spectral index γ = 3.42 ± 0.02. On the other hand, at low energies the measurements by C...
متن کاملKlein - Nishina steps in the energy spectrum of galactic cosmic ray electrons
The full Klein-Nishina cross section for the inverse Compton scattering interactions of electrons implies a significant reduction of the electron energy loss rate compared to the Thomson limit when the electron energy exceeds the critical Klein-Nishina energy E K = γ K m e c 2 = 0.27m 2 e c 2 /(k B T), where T denotes the temperature of the photon graybody distribution. As a consequence the tot...
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ژورنال
عنوان ژورنال: Physical Review Letters
سال: 1965
ISSN: 0031-9007
DOI: 10.1103/physrevlett.15.93